Chen, F.; Peter, H.; Bingert, S.; Cheung, M. C. M.: A model for the formation of the active region corona driven by magnetic flux emergence. Astronomy and Astrophysics 564, A12 (2014)
Bourdin, P.-A.; Bingert, S.; Peter, H.: Observationally driven 3D magnetohydrodynamics model of the solar corona above an active region. Astronomy and Astrophysics 555, A123 (2013)
Peter, H.; Bingert, S.; Klimchuk, J. A.; de Forest, C.; Cirtain, J. W.; Golub, L.; Winebarger, A. R.; Kobayashi, K.; Korreck, K. E.: Structure of solar coronal loops: from miniature to large-scale. Astronomy and Astrophysics 556, A104 (2013)
van Wettum, T.; Bingert, S.; Peter, H.: Parameterisation of coronal heating: spatial distribution and observable consequences. Astronomy and Astrophysics 554, A39 (2013)
Zacharias, P.; Peter, H.; Bingert, S.: Investigation of mass flows in the transition region and corona in a three-dimensional numerical model approach. Astronomy and Astrophysics 531, A97 (2011)
Bingert, S.; Peter, H.: Nanoflare Heating in the Solar Corona. In: High Performance Computing in Science and Engineering 14, pp. 113 - 120 (Eds. Nagel, W. E.; Kröner, D. H.; Resch, M. M.). Springer International Publishing, Switzerland (2015)
Chen, F.; Peter, H.; Bingert, S.: Magnetic Field Lines and Coronal Loops A Difficult Relation. Living With a Star / Iris / Hinode Meeting, Portland, USA (2014)
Chen, F.; Peter, H.; Bingert, S.; Cheung, M. C. M.: Magnetic field lines and coronal loops. 14th European Solar Physics Meeting, Dublin, Ireland (2014)
How does our star heat its outer atmosphere, the solar corona, to unimaginable temperatures of up to 10 million degrees Celsius? With unprecedented observational data from ESA's Solar Orbiter spacecraft and powerful computer simulations, ERC starting grant awardee Pradeep Chitta intends to bring new momentum to the search for the coronal heating mechanism.
The research group “Solar Lower Atmosphere and Magnetism” (SLAM) studies the conditions and dynamic processes in the atmospheric layer between the solar surface (photosphere) and the overlying chromosphere, an approximately 2000 km thick gas layer.
The main research fields of the department "Sun and Heliosphere" are covered by the research groups "Solar and Stellar Coronae", "Solar Lower Atmosphere and Magnetism", "Solar and Stellar Magnetohydrodynamics" and "Solar Variability and Climate".